The TPA census consists of 1267 pulsars and is fully described in [1]}. For the 21 interpulse pulsars in our sample, we performed independent fits on the main and interpulse components where sufficient PA points were available. Not all of the pulsars are amenable to RVM fitting. We required at least 10 PA points across the profile to proceed with the fit. This effectively removes pulsars for which the signal to noise ratio is low and pulsars which are bright but have very low level of linear polarization. In addition we removed pulsars which are scattered at our observing frequency as recorded in [2]}. Scattering has the effect of causing distortions in the PA swing due to the convolution of the Stokes Q and U profiles with an exponential function [3]}. These criteria led to a removal of 434 pulsars from the sample, listed in Table REF . This leaves a grand total of 854 RVM fit attempts.
